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The distribution and morphology of X-ray-emitting gas in the core of the Perseus clusterAn unresolved source has been found coincident with the nucleus of NGC 1275 in a high-resolution X-ray image of the core of the Perseus cluster. Absorption in the optical features at high velocity with respect to NGC 1275, which are thought to be associated with a foreground galaxy, does not produce any detectable X-ray absorption. The emission tends to become asymmetric in the presence of the lower-velocity filaments, but no obvious, detailed correlation is found between X-ray enhancements and individual filaments. Deprojection of surface brightness to yield temperature and density profiles of the intracluster gas shows results consistent with a quasi-hydrostatic radiative accretion flow onto NGC 1275, and the pressure-driven mass inflow onto the central galaxy is then 200-400 solar masses/yr. The possibility of a problem in the relation of line-of-sight velocity dispersion to cluster gravitational mass is confirmed.
Document ID
19810061726
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Fabian, A. C.
(Cambridge University Cambridge, United Kingdom)
Hu, E. M.
(Carnegie Institution of Washington Washington, DC, United States)
Cowie, L. L.
(Princeton University New Observatory, Princeton, NJ, United States)
Grindlay, J.
(Cambridge Univ. Cambridge, United Kingdom)
Date Acquired
August 11, 2013
Publication Date
August 15, 1981
Publication Information
Publication: Astrophysical Journal
Subject Category
Astrophysics
Accession Number
81A46130
Funding Number(s)
CONTRACT_GRANT: NGL-31-001-007
CONTRACT_GRANT: NAS8-33345
Distribution Limits
Public
Copyright
Other

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